Radio morphology of the remnant radio galaxy in A2065 shows that it is an elongated, bar-shaped structure (52\(^{\prime \prime }\)  \(\times \)  110\(^{\prime \prime }\)  \(\simeq \)  72 \(\times \)  152 kpc\(^2\) ), which is buried within a radio halo emission of size \(\lesssim \)  1 Mpc in size [1]} and [2]}.
The remnant radio galaxy is located in the near vicinity of the southern cD galaxy; the northeastern boundary of the remnant radio galaxy is merely at a distance of \(\sim \) 33\(^{\prime \prime }\)  (\(\simeq \)  45.7 kpc) from the southern cD galaxy.
The possible radio core of the remnant radio galaxy is coincident with the WISEA J152228.01\(+\) 274141.3 source that is 78 away from the optical galaxy V1CG 136.
Our spectral index measurements show that the radio spectrum steepens with distance from the possible radio core from \(\alpha \)  = \(-\) 1.2 \(\pm \) 0.1 to \(\alpha \)  = \(-\) 1.4 \(\pm \) 0.2 in our low-frequency (between the 240 MHz band and the 250–500 MHz band) spectra, and from \(\alpha \)  = \(-\) 1.3 \(\pm \) 0.1 to \(\alpha \)  = \(-\) 1.6 \(\pm \) 0.2 in our high-frequency (between the 250–500 MHz band and the 610 MHz band) spectra (Figure REF ), as is expected for synchrotron and inverse Compton losses. We also find evidence for spectral steepening across the remnant radio galaxy in our in-band spectral index measurements, from \(\alpha \)  = \(-\) 1.3 \(\pm \) 0.2 to \(\alpha \)  = \(-\) 1.4 \(\pm \) 0.2 (Figure REF ), in the direction away from the two cD galaxies.
Our X-ray measurements show a surface-brightness edge that is coincident with the northeastern boundary of the remnant radio galaxy and its nature (shock or cold front) is not clear from the data. If it is a shock front, it is rather weak, with \(M\)  being between 1.1 and 1.3; however it is unclear if an (inward?) traveling shock is responsible for spectral steepening across the remnant radio galaxy.
Below we discuss the possible progenitor of the remnant radio galaxy in A2065.
